We present an analysis of a newly discovered 2+1+1 quadruple system with TESS
containing an unresolved eclipsing binary (EB) as part of TIC 121088960 and a
close neighbor TIC 121088959. The EB consists of two very low-mass M dwarfs in
a highly-eccentric ($e$ = 0.709) short-period ($P$ = 3.04358 d) orbit. Given
the large pixel size of TESS and the small separation (3.9$"$) between TIC
121088959 and TIC 121088960, we used light centroid analysis of the difference
image between in-eclipse and out-of-eclipse data to show that the EB likely
resides in TIC 121088960, but contributes only $\sim$10% of its light. Radial
velocity data were acquired with iSHELL at NASA's Infrared Facility and the
Coud$é$ spectrograph at the McDonald 2.7-m telescope. For both images, the
measured RVs showed no variation over the 11-day observational baseline, and
the RV difference between the two images was $8 0.3$ km s$^-1$. The
similar distances and proper motions of the two images indicate that TIC
121088959 and TIC 121088960 are a gravitationally bound pair. Gaia's large RUWE
and astrometric_excess_noise parameters for TIC 121088960, further indicate
that this image is the likely host of the unresolved EB and is itself a triple
star. We carried out an SED analysis and calculated stellar masses for the four
stars, all of which are in the M dwarf regime: 0.19 M$_ødot$ and 0.14
M$_ødot$ for the EB stars and 0.43 M$_ødot$ and 0.39 M$_ødot$ for the
brighter visible stars, respectively. Lastly, numerical simulations show that
the orbital period of the inner triple is likely the range 1 to 50 years.
Описание
A 2 1 1 quadruple star system containing the most eccentric, low-mass, short-period, eclipsing binary known
%0 Generic
%1 han2021quadruple
%A Han, E.
%A Rappaport, S. A.
%A Vanderburg, A.
%A Tofflemire, B. M.
%A Borkovits, T.
%A Schwengeler, H. M.
%A Zasche, P.
%A Krolikowski, D. M.
%A Muirhead, P. S.
%A Kristiansen, M. H.
%A Terentev, I. A.
%A Omohundro, M.
%A Gagliano, R.
%A Jacobs, T.
%A LaCourse, D.
%D 2021
%K mdwarf multiplicity
%T A 2+1+1 quadruple star system containing the most eccentric, low-mass,
short-period, eclipsing binary known
%U http://arxiv.org/abs/2112.00028
%X We present an analysis of a newly discovered 2+1+1 quadruple system with TESS
containing an unresolved eclipsing binary (EB) as part of TIC 121088960 and a
close neighbor TIC 121088959. The EB consists of two very low-mass M dwarfs in
a highly-eccentric ($e$ = 0.709) short-period ($P$ = 3.04358 d) orbit. Given
the large pixel size of TESS and the small separation (3.9$"$) between TIC
121088959 and TIC 121088960, we used light centroid analysis of the difference
image between in-eclipse and out-of-eclipse data to show that the EB likely
resides in TIC 121088960, but contributes only $\sim$10% of its light. Radial
velocity data were acquired with iSHELL at NASA's Infrared Facility and the
Coud$é$ spectrograph at the McDonald 2.7-m telescope. For both images, the
measured RVs showed no variation over the 11-day observational baseline, and
the RV difference between the two images was $8 0.3$ km s$^-1$. The
similar distances and proper motions of the two images indicate that TIC
121088959 and TIC 121088960 are a gravitationally bound pair. Gaia's large RUWE
and astrometric_excess_noise parameters for TIC 121088960, further indicate
that this image is the likely host of the unresolved EB and is itself a triple
star. We carried out an SED analysis and calculated stellar masses for the four
stars, all of which are in the M dwarf regime: 0.19 M$_ødot$ and 0.14
M$_ødot$ for the EB stars and 0.43 M$_ødot$ and 0.39 M$_ødot$ for the
brighter visible stars, respectively. Lastly, numerical simulations show that
the orbital period of the inner triple is likely the range 1 to 50 years.
@misc{han2021quadruple,
abstract = {We present an analysis of a newly discovered 2+1+1 quadruple system with TESS
containing an unresolved eclipsing binary (EB) as part of TIC 121088960 and a
close neighbor TIC 121088959. The EB consists of two very low-mass M dwarfs in
a highly-eccentric ($e$ = 0.709) short-period ($P$ = 3.04358 d) orbit. Given
the large pixel size of TESS and the small separation (3.9$"$) between TIC
121088959 and TIC 121088960, we used light centroid analysis of the difference
image between in-eclipse and out-of-eclipse data to show that the EB likely
resides in TIC 121088960, but contributes only $\sim$10% of its light. Radial
velocity data were acquired with iSHELL at NASA's Infrared Facility and the
Coud${\'e}$ spectrograph at the McDonald 2.7-m telescope. For both images, the
measured RVs showed no variation over the 11-day observational baseline, and
the RV difference between the two images was $8 \pm 0.3$ km s$^{-1}$. The
similar distances and proper motions of the two images indicate that TIC
121088959 and TIC 121088960 are a gravitationally bound pair. Gaia's large RUWE
and astrometric_excess_noise parameters for TIC 121088960, further indicate
that this image is the likely host of the unresolved EB and is itself a triple
star. We carried out an SED analysis and calculated stellar masses for the four
stars, all of which are in the M dwarf regime: 0.19 M$_\odot$ and 0.14
M$_\odot$ for the EB stars and 0.43 M$_\odot$ and 0.39 M$_\odot$ for the
brighter visible stars, respectively. Lastly, numerical simulations show that
the orbital period of the inner triple is likely the range 1 to 50 years.},
added-at = {2021-12-02T15:53:21.000+0100},
author = {Han, E. and Rappaport, S. A. and Vanderburg, A. and Tofflemire, B. M. and Borkovits, T. and Schwengeler, H. M. and Zasche, P. and Krolikowski, D. M. and Muirhead, P. S. and Kristiansen, M. H. and Terentev, I. A. and Omohundro, M. and Gagliano, R. and Jacobs, T. and LaCourse, D.},
biburl = {https://www.bibsonomy.org/bibtex/2c37e69aed066f59a4498100898860488/superjenwinters},
description = {A 2 1 1 quadruple star system containing the most eccentric, low-mass, short-period, eclipsing binary known},
interhash = {f24bf64e2059089da51798ca5d99beb2},
intrahash = {c37e69aed066f59a4498100898860488},
keywords = {mdwarf multiplicity},
note = {cite arxiv:2112.00028},
timestamp = {2021-12-02T15:53:21.000+0100},
title = {A 2+1+1 quadruple star system containing the most eccentric, low-mass,
short-period, eclipsing binary known},
url = {http://arxiv.org/abs/2112.00028},
year = 2021
}